THE GLOBAL STRUCTURE OF THE INFLATIONARY UNIVERSE

1987 ◽  
Vol 02 (03) ◽  
pp. 561-591 ◽  
Author(s):  
A. S. GONCHAROV ◽  
A. D. LINDE ◽  
V. F. MUKHANOV

In this article we give a review of recent results concerning the global structure of the inflationary universe, which have been obtained within stochastic approach to inflation. It is shown in particular that the evolution of the universe in the chaotic inflation scenario has no end and may have no beginning. In this scenario the major part of the physical volume of the universe always remains in the inflationary phase. During inflation the universe becomes divided into many exponentially large domains, inside which all possible metastable vacuum states and all possible types of compactification compatible with inflation are realized.

1986 ◽  
Vol 01 (02) ◽  
pp. 81-85 ◽  
Author(s):  
A.D. LINDE

It is shown that the evolution of the universe in the chaotic inflation scenario has no end and may have no beginning. According to this scenario, the universe consists of an exponentially large number of different mini-universes inside which all possible metastable vacuum states and all possible types of compactifications are realized.


1994 ◽  
Vol 03 (01) ◽  
pp. 23-30
Author(s):  
NATHALIE DERUELLE ◽  
DAVID LANGLOIS ◽  
DAVID POLARSKI

We sketch the logics of the argument which claims that the temperature fluctuations in the microwave background radiation, observed by the COBE satellite, have originated from quantum vacuum fluctuations in an early, inflationary phase of the evolution of the universe.


2018 ◽  
Vol 27 (05) ◽  
pp. 1850052 ◽  
Author(s):  
Jaume Haro ◽  
Supriya Pan

In a spatially-flat Friedmann–Lemaître–Robertson–Walker universe, the incorporation of bulk viscous process in general relativity leads to an appearance of a nonsingular background of the universe that both at early and late times depicts an accelerated universe. These early and late scenarios of the universe can be analytically calculated and mimicked, in the context of general relativity, by a single scalar field whose potential could also be obtained analytically where the early inflationary phase is described by a one-dimensional Higgs potential and the current acceleration is realized by an exponential potential. We show that the early inflationary universe leads to a power spectrum of the cosmological perturbations which match with current observational data, and after leaving the inflationary phase, the universe suffers a phase transition needed to explain the reheating of the universe via gravitational particle production. Furthermore, we find that at late times, the universe enters into the de Sitter phase that can explain the current cosmic acceleration. Finally, we also find that such bulk viscous-dominated universe attains the thermodynamical equilibrium, but in an asymptotic manner.


2003 ◽  
Vol 18 (29) ◽  
pp. 2039-2049 ◽  
Author(s):  
Víctor H. Cárdenas ◽  
Sergio del Campo ◽  
Ramón Herrera

Scalar density cosmological perturbations, spectral indices and reheating in a chaotic inflationary universe model, in which a higher derivative term is added, are investigated. This term is supposed to play an important role in the early evolution of the Universe, specifically at times closer to the Planck era.


2012 ◽  
Vol 27 (04) ◽  
pp. 1250014 ◽  
Author(s):  
PAVAN K. ALURI ◽  
PANKAJ JAIN

We show that perturbations generated during the anisotropic pre-inflationary stage of cosmic evolution may affect cosmological observations today for a certain range of parameters. Due to the anisotropic nature of the universe during such early times, it might explain some of the observed signals of large scale anisotropy. In particular, we argue that the alignment of CMB quadrupole and octopole may be explained by the Sachs–Wolfe effect due to the large scale anisotropic modes from very early times of cosmological evolution. We also comment on how the observed dipole modulation of CMB power may be explained within this framework.


Think ◽  
2021 ◽  
Vol 21 (60) ◽  
pp. 33-49
Author(s):  
William Lyons

The author sets out to respond to the student complaint that ‘Philosophy did not answer “the big questions”’, in particular the question ‘What is the meaning of life?’ The response first outlines and evaluates the most common religious answer, that human life is given a meaning by God who created us and informs us that this life is just the pilgrim way to the next eternal life in heaven. He then discusses the response that, from the point of view of post-Darwinian science and the evolution of the universe and all that is in it, human life on Earth must be afforded no more meaning than the meaning we would give to a microscopic planaria or to some creature on another planet in a distant universe. All things including human creatures on Planet Earth just exist for a time and that is that. There is no plan or purpose. In the last sections the author outlines the view that it is we humans ourselves who give meaning to our lives by our choices of values or things that are worth pursuing and through our resulting sense of achievement or the opposite. Nevertheless the question ‘What is the meaning of life?’ can mean quite different things in different contexts, and so merit different if related answers. From one point of view one answer may lie in terms of the love of one human for another.


2021 ◽  
pp. 2150111
Author(s):  
Fei-Quan Tu ◽  
Bin Sun ◽  
Meng Wan ◽  
Qi-Hong Huang

Entropy is a key concept widely used in physics and other fields. At the same time, the meaning of entropy with different names and the relationship among them are confusing. In this paper, we discuss the relationship among the Clausius entropy, Boltzmann entropy and information entropy and further show that the three kinds of entropy are equivalent to each other to some extent. Moreover, we point out that the evolution of the universe is a process of entropy increment and life originates from the original low entropy of the universe. Finally, we discuss the evolution of the entire universe composed of the cosmological horizon and the space surrounded by it and interpret the entropy as a measure of information of all microstates corresponding to a certain macrostate. Under this explanation, the thermodynamic entropy and information entropy are unified and we can conclude that the sum of the entropy of horizon and the entropy of matter in the space surrounded by the horizon does not decrease with time if the second law of thermodynamics holds for the entire universe.


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